Science Lessons Learned from TESIS and their Relevance to SWAP

V. Slemzin, LPI

PROBA 2 SWT, La Roche, 14 June 2010

TESIS scientific team (LPI):S. Kuzin, S. Bogachev, S. Shestov, V. Slemzin, A. Ulyanov, A. Reva

CORONAS-Photon was launched on January 31, 2009

The projected time of the mission was 2 years

The flight was terminated after 9 months in November 2009 because of problems with the satellite power system. TESIS

Array of TESIS instruments

CHANNELS (7)

MgXIIMgXII

8.42 A8.42 A

Telescope 1Telescope 1

132 A132 A

FeXX-XXIIIFeXX-XXIII

Telescope 2Telescope 2

171/304 A171/304 A

FeIX-X / He IIFeIX-X / He II

CORONO-CORONO-GRAPHGRAPH

304A304A

SPECTRO-HELIOSPECTRO-HELIO

GRAPHGRAPH

SphinX SphinX photometer photometer SRC PANSRC PAN

SpectralRange, A

8.41-8.42

131-132

171-178 295-315

295-315

285-335

1-12

Fieldof View

45’ Disk: 10

Corona: 2-5 Rsun

2.5° ~2° -

AngularResolution

3” 1.7” 20”  X: 1.7”Y: 40”

-

SpectralResolution

0.0002 A/pixel

70 20 20 0.01 A/pixel ~0.05

Exposition,sec

0.01-600 0.01-0.001

TESIS: parameters of EUV telescopes

Wavelength band 132 A (telescope I)

171 / 304 A (telescope II) Focal length……………. 1600 mm Mirror Aperture…...100 mm diameter Field of view ……………………... 1° Angular resolution……1.7 arc sec/pix Max. cadence…………1 sec (partial frame)

10 sec (full frame)

Typical cadence………..2 – 5 min Detector……….… backside CCD

2048 × 2048 pixels

CORONAS-Photon orbit

01.01.2010 01.07.2010 01.01.20110,4

0,6

0,8

1,0

no

n-o

bsc

ure

d v

iew

, % o

f the

orb

it

CORONAS-Photon

PROBA 2

Horb =550-570 km, α = 820

Eclipse time for one 95 min orbit

TESIS resuls1. Eruption of giant prominences in 304 A

TESIS HeII 304 A 23/04-2009

2. Dynamics of active regions in 171 A

3. Short-time dynamics

Nanoflares in 171 A

Cadence 3 s, exposure 0.5 s

Dynamics of spicules in 304 A

4. Eruption of a giant prominence in 304 A and U-shaped magnetic feature

12 May 2009

4. Quasi-static inner corona in 171 A

Overexposure (10 s instead of 0.1s)

Low straylight (one-mirror telescope)

Coronal dynamics during one solar rotation1-27 September 2009

N W S E N

TESIS lessons The scientific program was not fulfilled because the mission was

terminated in November 2009 due to failure of the satellite power system. Total volume of information: 700 Gb, 150000 images.

In 2009 the solar activity was unexpectedly low. Two high temperature channels did not provide valuable data (Mg, 132 A)

At very low solar activity there are many specific phenomena as global and small scale: eruption of giant prominences, a lot of bright EUV points, rich magnetic structure of the inner corona, reconnection of closed structures with open interplanetary lines.

The 171 A band is very informative to study the inner corona (T ~ 1-2 MK) in global and local scales.

Perspectives: EUV imaging with resolution < 1” and cadence of 1 s (“Arka” project)

Level 1 TESIS data are available at http://www.tesis.lebedev.ru/en/data_access.html

The inner corona in SWAP

1x10s 100x10s equatorial scan

100x10s

N W S E N

1x10s

SWAP – LASCO C2